Modeling of fluid flow in pipeline and the difference scheme stability investigation

A mathematical model of viscous fluid flow in the pipeline with the presence of flow across the surface and the narrowing of pipeline section, which is based on a system of Navier-Stokes equations in two-dimensional rectangular region with a special type of boundary conditions has been designed. The geometric configuration of the leakage zone is taken into the account. It is believed that the fluid motion is under the influence of constant length of pressure difference. For the solving of this system, the numerical method of finite differences was developed by which the finite differences scheme is realized – the first step is implicit in longitudinal coordinate, and the second – on the transversal. The study on the stability of the spectral features method, stability conditions are established for the case of flow calculation with specified parameters and for the given type of the pipeline geometry. The criterion of numerical stability is presented taking to account the model’s parameters.Побудовано математичну модель течії в’язкої рідини в трубопроводі за наявності перетікання рідини через поверхню та звуження поперечного перерізу, яка базується на системі рівнянь Нав’є – Стокса в двовимірній прямокутній системі координат зі спеціальним типом граничних умов. Враховано просторову конфігурацію зон перетікання. Рух рідини здійснюється під дією постійного перепаду тиску по довжині труби. Для розв’язання задачі використано метод скінчених різниць, розроблено чисельний метод його реалізації – перший крок ітераційного процесу здійснюється по повздовжній, другий – по поперечній координатах. Вивчення стійкості проводиться за спектральною ознакою, встановлено умови стійкості для розрахунку течії зі спеціальними параметрами і для заданого типу геометрії труби. Критерії стійкості розрахунків представлено з урахуванням параметрів моделі.Построено математическую модель течения вязкой жидкости в трубопроводе при наличии перетекания жидкости через поверхность и сужения поперечного сечения, основанная на использовании двухмерной системе уравнений Навье – Стокса в прямоугольной системе координат со специальным типом граничних условий. Учтена пространственная конфигурация зон перетекания. Движение жидкости обусловлено постоянным перепадом давления по длине трубы. Для решения задачи используется метод конечних різностей, создан численный метод его реализации – первуй шаг итерационного процесса осуществляется по продольной, второй – по поперечной координатах. Изучение устойчивости проводится с использованим спектрального признака устойчивости, установлены условия устойчивости для расч.та течений со специальными параметрами и для данного типа геометрии трубы. Критерии устойчивости представлены с уч.том параметров модели

Macro-Economic and Bank-Specific Determinants of Credit Risk in Commercial Banks

Inadequate credit risk assessment procedures may have a significant negative influence on a financial institution's operational performance, perhaps leading to liquidity concerns.  It is hypothesized that different factors such as macroeconomic, and bank-specific factors affect the credit risk in financial institutions. The objective of this study is to check those factors responsible for credit risk. The data came from WDI and Bankscope databases. The data is balanced panel data of 106 private and state-owned commercial banks for 6 years (n=106, t=6). This study used Fixed Effect (FE), and Random Effect (RE) models. The results suggest that if inflation, interest rate, unemployment increase, the credit risk of commercial banks increases. The results also suggest that if GDP growth, efficiency, and bank size increase, the credit risk become minimized. Additionally, the credit risk is lower in private banks than in state-owned banks. The findings of this research, however, do not support the hypotheses that exchange rate and regulatory capitals influence credit risk

Rest-frame ultraviolet-to-optical spectral characteristics of extremely metal-poor and metal-free galaxies

Finding the first generation of galaxies in the early Universe is the greatest step forward for understanding galaxy formation and evolution. For strategic survey of such galaxies and interpretation of the obtained data, this paper presents an ultraviolet-to-optical spectral model of galaxies with a great care of the nebular emission. In particular, we present a machine-readable table of intensities of 119 nebular emission lines from Ly$\alpha$ to the rest-frame 1 $\mu$m as a function of metallicity from zero to the Solar one. Based on the spectral model, we present criteria of equivalent widths of Ly$\alpha$, He {\sc ii} $\lambda1640$, H$\alpha$, H$\beta$, [O {\sc iii}] $\lambda5007$ to select extremely metal-poor and metal-free galaxies although these criteria have uncertainty caused by the Lyman continuum escape fraction and the star formation duration. We also present criteria of broad-band colours which will be useful to select candidates for spectroscopic follow-up from drop-out galaxies. We propose the line intensity ratio of [O {\sc iii}] $\lambda5007$ to H$\beta$ $<0.1$ as the most robust criterion for $<1/1000$ of the Solar metallicity. This ratio of a galaxy with a few $M_\odot$ yr$^{-1}$ at $z\sim8$ is detectable by spectroscopy with the James Webb Space Telescope within a reasonable exposure time.Comment: 13 pages, 14 figures, MNRAS in press. Emission line emissivities are available at http://www.las.osaka-sandai.ac.jp/~inoue/EMPgalspec/Line.tg

The regeneration of a weak acid action exchanger with an aequeous solution of sulphurdioxide

A dissertation submitted to the Faculty of Engineering, University of the Witwatersrand, in fu lfilm e n t o f the requirements for the degree of Master of Science in Engineering by Paul R a iter, B.Sc. (Eng,) Johannesburg September

An implementation of sharpe’s capital asset pricing model

This paper implements computationally Sharpe (1964) Capital Asset Pricing Model (CAPM) in order to provide a script that collects data, calculates the parameters of CAPM and tests the statistical significance of those parameters for any asset traded in Brazilian Stock Exchange (B3). The model is estimated using Brazilian’s interbank interest rate (CDI) as the risk free return and B3 stock market index (Ibovespa) return as a proxy for market return. We implemented the CAPM by using Python programming language and tested the program operation for a subset of B3 stock market assets. The results has shown the application was able to attend all functional requirements and, in addition, it is amenable to be developed to provide new features such as parameters of international capital asset pricing model as stated in Frankel (1982).Esse artigo implementa computacionalmente Sharpe (1964) Capital Asset Pricing Model (CAPM) com o objetivo de prover uma aplicação que coleta dados, calcula os parâmetros do CAPM e testa a significância estatística desses parâmetros para qualquer ação negociada na bolsa de valores brasileira (B3). O modelo é estimado utilizando o Certificado de Depósito Interbancário como a taxa livre de risco e o Ibovespa como uma proxy para o retorno de mercado. Nós implementamos o CAPM utilizando a linguagem de programação Python e testamos a operação do programa para um conjunto de ações da B3. Os resultados mostraram que a aplicação foi capaz de atender todos os requerimentos funcionais e, em adição, é passível de desenvolvimento para prover novas funcionalidades, como parâmetros do CAPM internacional como exposto em Frankel (1982)

The nature of z ~ 2.3 Lyman-alpha emitters

We study the multi-wavelength properties of a set of 171 Ly-alpha emitting candidates at redshift z = 2.25 found in the COSMOS field, with the aim of understanding the underlying stellar populations in the galaxies. We especially seek to understand what the dust contents, ages and stellar masses of the galaxies are, and how they relate to similar properties of Ly-alpha emitters at other redshifts. The candidates here are shown to have different properties from those of Ly-alpha emitters found at higher redshift, by fitting the spectral energy distributions (SEDs) using a Monte-Carlo Markov-Chain technique and including nebular emission in the spectra. The stellar masses, and possibly the dust contents, are higher, with stellar masses in the range log M_* = 8.5 - 11.0 M_sun and A_V = 0.0 - 2.5 mag. Young population ages are well constrained, but the ages of older populations are typically unconstrained. In 15% of the galaxies only a single, young population of stars is observed. We show that the Ly-alpha fluxes of the best fit galaxies are correlated with their dust properties, with higher dust extinction in Ly-alpha faint galaxies. Testing for whether results derived from a light-weighted stack of objects correlate to those found when fitting individual objects we see that stellar masses are robust to stacking, but ages and especially dust extinctions are derived incorrectly from stacks. We conclude that the stellar properties of Ly-alpha emitters at z = 2.25 are different from those at higher redshift and that they are diverse. Ly-alpha selection appears to be tracing systematically different galaxies at different redshifts.Comment: 15 pages, 11 figures, 8 tables, accepted in A&A. Table 6 available in full from the author

Effects of Star Formation Stochasticity on the Ly-alpha & Lyman Continuum Emission from Dwarf Galaxies during Reionization

Observations of distant galaxies play a key role in improving our understanding of the Epoch of Reionization (EoR). The observed Ly-alpha emission line strength - quantified by its restframe equivalent width (EW) - provides a valuable diagnostic of stellar populations and dust in galaxies during and after the EoR. In this paper we quantify the effects of star formation stochasticity on the predicted Ly-alpha EW in dwarf galaxies, using the publicly available code SLUG ('Stochastically Light Up Galaxies'). We compute the number of hydrogen ionizing photons, as well as flux in the Far UV for a set of models with star formation rates (SFR) in the range 10-3-1 Msol/yr. From these fluxes we compute the luminosity, L-alpha, and the EW of the Ly-alpha line. We find that stochasticity alone induces a broad distribution in L-alpha and EW at a fixed SFR, and that the widths of these distributions decrease with increasing SFR. We parameterize the EW probability density function (PDF) as an SFR-dependent double power law. We find that it is possible to have EW as low as ~EW0/4 and as high as ~3 times the EW0, where EW0 denotes the expected EW in the absence of stochasticity. We argue that stochasticity may therefore be important when linking drop-out and narrow-band selected galaxies, when identifying population III galaxies, and that it may help to explain the large EW (EW > 100 - 200 A) observed for a fraction of Ly-alpha- selected galaxies. Finally, we show that stochasticity can also affect the inferred escape fraction of ionizing photons from galaxies. In particular, we argue that stochasticity may simultaneously explain the observed anomalous ratios of the Lyman continuum flux density to the (non-ionizing) UV continuum density in so-called Lyman-Bump galaxies at z = 3.1, as well as the absence of such objects among a sample of z = 1.3 drop-out galaxies.Comment: 9 pages, 4 figures, accepted for publication in MNRA

La paradoja de lo público.

Fil: Raiter, Alejandro. Universidad de Buenos Aires; Argentina8 ref.En este trabajo nos proponemos explorar uno de los aspectos del fenómeno social descripto por Habermas (1985): los ciudadanos no actúan racionalmente en el capitalismo tardío. Utilizaremos el análisis del discurso para mostrar que los textos periodísticos no están funcionando para facilitar el acceso de los ciudadanos a la información necesaria para actuar; por el contrario, proveen información que impide la toma de la decisión individual de actuar. Utilizaremos un pequeño corpus extraído del suplemento económico "Cash" del diario Página 12 para ejemplificar nuestra afirmación y analizaremos el lugar de enunciación del texto periodístico comparandolo con el del discurso científico y el discurso histórico

Detecting gravitationally lensed population III galaxies with the Hubble Space Telescope and the James Webb Space Telescope

Small galaxies consisting entirely of population III (pop III) stars may form at high redshifts, and could constitute one of the best probes of such stars. Here, we explore the prospects of detecting gravitationally lensed pop III galaxies behind the galaxy cluster J0717.5+3745 (J0717) with both the Hubble Space Telescope (HST) and the upcoming James Webb Space Telescope (JWST). By projecting simulated catalogs of pop III galaxies at z~7-15 through the J0717 magnification maps, we estimate the lensed number counts as a function of flux detection threshold. We find that the ongoing HST survey CLASH, targeting a total of 25 galaxy clusters including J0717, potentially could detect a small number of pop III galaxies if ~1% of the baryons in these systems have been converted into pop III stars. Using JWST exposures of J0717, this limit can be pushed to ~0.1% of the baryons. Ultra-deep JWST observations of unlensed fields are predicted to do somewhat worse, but will be able to probe pop III galaxies with luminosities intermediate between those detectable in HST/CLASH and in JWST observations of J0717. We also explain how current measurements of the galaxy luminosity function at z=7-10 can be used to constrain pop III galaxy models with very high star formation efficiencies (~10% of the baryons converted into pop III stars).Comment: 14 pages, 7 figures, accepted for publication in MNRAS (v.2: presentation improved, but only minor changes in overall results

Pair-Instability Supernovae at the Epoch of Reionization

Pristine stars with masses between ~140 and 260 M_sun are theoretically predicted to die as pair-instability supernovae. These very massive progenitors could come from Pop III stars in the early universe. We model the light curves and spectra of pair-instability supernovae over a range of masses and envelope structures. At redshifts of reionization z >= 6, we calculate the rates and detectability of pair-instability and core collapse supernovae, and show that with the James Webb Space Telescope, it is possible to determine the contribution of Pop III and Pop II stars toward reionization by constraining the stellar initial mass function at that epoch using these supernovae. We also find the rates of Type Ia supernovae, and show that they are not rare during reionization, and can be used to probe the mass function at 4-8 M_sun. If the budget of ionizing photons was dominated by contributions from top-heavy Pop III stars, we predict that the bright end of the galaxy luminosity function will be contaminated by pair-instability supernovae.Comment: 12 pages, 11 figures. Matches MNRAS accepted versio